| NGC 5846 | |
|---|---|
 NGC 5846 (right) andNGC 5850 (left) by the Schulman Telescope atMount Lemmon SkyCenter | |
| Observation data (J2000epoch) | |
| Constellation | Virgo |
| Right ascension | 15h 06m 29.3s[1] |
| Declination | +01° 36′ 20″[1] |
| Redshift | 0.005711 ± 0.000017[1] |
| Heliocentric radial velocity | 1,712 ± 5km/s[1] |
| Distance | 93 ± 32Mly (28.5 ± 9.8Mpc)[1] |
| Apparent magnitude (V) | 10.1[2] |
| Characteristics | |
| Type | E0-1[1] |
| Apparent size (V) | 4′.1 × 3′.8 |
| Notable features | StrongX-ray source |
| Other designations | |
| UGC 9706,CGCG 020-061,MCG +00-38-025,PGC 53932[1] | |
NGC 5846 is anelliptical galaxy located in the constellationVirgo. It is located at a distance of circa 90 millionlight years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered byWilliam Herschel on February 24, 1786.[3] It lies near110 Virginis and is part of theHerschel 400 Catalogue.[4] It is a member of theNGC 5846 Group of galaxies, itself one of theVirgo III Groups strung out to the east of theVirgo Supercluster of galaxies.[5]
NGC 5846 is a giant elliptical galaxy with a round shape. It has a low luminosityactive galactic nucleus, whose categorisation is ambiguous, having features that are observed both inLINER andHII regions.[6] The source of nuclear activity in galaxies is suggested to be asupermassive black hole that accretes material. NGC 5846 harbors a supermassive black hole with estimated mass(1.1±0.1)×109 M☉ based on the centralvelocity dispersion.[7][8]
NGC 5846 harbors a large number ofglobular clusters; over 1,200 have been detected in images byHubble Space Telescope.[9] The specific frequency is similar to other elliptical galaxies in groups. As has been observed in other large elliptical galaxies, themetallicity has bimodial distribution, with metallicities roughly of [Fe/H]=-1.2 and -0.2.[10] Their typical effective radii are in the range of 3 - 5 pc, with the largest clusters located in the central regions. Seven of the globular clusters have X-ray counterparts, which are among the most luminous X-ray sources in NGC 5846. These clusters are mostly in the central region and they are optically luminous, compact and belong to the red subpopulation.[11]
The galaxy has complex X-ray morphology[13] that is considered to be the result of AGN outflows. Two inner bubbles in the hot gas, at a distance of 600 pc from the center and filled with radio emission, are clear indications of recent AGN feedback. A weak radio source, elongated in the NE–SW direction, connects the inner cavities. X-ray-bright rims surround the inner X-ray bubbles.[7] Many X-ray knots are visible, suggesting cooling sites. The scenario indicated by the Chandra observation is that of an AGN outflow, compressing and cooling the gas[14] in the central ~2 kpc (20" at the distance of NGC 5846).[12]
Hα observations[13][15][16] reveal the presence of warmionized gas in the inner 2 kpc of NGC 5846. Spectra of this gas indicate irregular motion, with a typical velocity of 150–200 km s−1. The warm gas traces the X-ray-bright features, again suggesting a multiphase AGN outflow.[12] Using theSpitzer IRS[17] mid-infrared lines were detected (e.g., [Ne ii] 12.81 μm, [Ne iii] 15.55 μm) but no trace ofpolycyclic aromatic hydrocarbon (PAH) emission. Several sources are identified in the radio at 2.3, 5, and 15 GHz using VLBA data; these sources are aligned in the south–north direction.[18]
RecentHerschel PACS observations have detected the presence of [C ii]-emitting gas that extends to a radius of ~2 kpc and is centrally peaked. The [C ii] emission is almost exactly cospatial with the H-alpha +[N II] emission, and the total fluxes in [C ii] and H-alpha +[N II] have a ratio of 2.5, a very similar flux ratio value observed in other group-centered ellipticals.[16] Furthermore, the velocities inferred from the [C ii] line are consistent with those measured for the Hα line.[15] All of this evidence suggests that the [C ii] line is emitted by the warm gas, and it is not necessarily tracing the molecular phase.[12]
NGC 5846 has another indication that the cold gas is being disturbed by an AGN outburst. It has, in fact, an excess of cold (T ~ 30 K) dust approximately cospatial with the ionized and molecular gas. With a 70 μm luminosity of 3.5 × 1041 erg s−1,[19] NGC 5846 shares the same dust properties as several giant ellipticals (e.g.,NGC 4636 andNGC 5044[20]), which are best explained with the ejection of dusty gas from their centers by AGN activity that occurred ~107 yr ago.[12]
ThreeCO clouds have been detected in NGC 5846. Clouds 1 and 3 are resolved in at least one direction byALMA 12 m array observations and extend to 1"2 and 2"9, respectively, and are about 5"5 and 8"4 away (0.6 and 1.0 kpc) from the galaxy center, respectively. Cloud 3 is aligned almost exactly along a dust filament, while cloud 1 also coincides with small dust extinction structures. The elongation and potential bimodality of the surface brightness of cloud 3 of NGC 5846 could indicate that it might be composed of two nearby (in projection) clouds. Cloud 2 lies further away from the centre and is thought to originate from cooling in the wakes beneath buoyant X-ray cavities where compressions stimulate significant large-scale, coherent radiative cooling.[12]
NGC 5846 forms a non-interacting pair withNGC 5846A, which lies 0.7 arcminutes from NGC 5846.[21] Its proximity to NGC 5846 and high surface brightness suggests it has beentidally stripped.[22] The barred spiral galaxyNGC 5850 lies at a projected distance of 10 arcminutes from NGC 5846 and may form an interacting pair with NGC 5846 based on its disturbed morphology. It is suggested that the two galaxies had a high speed encounter approximately 200 million years ago.[23]
NGC 5846 has a companion named NGC 5846-UDG1, an example of anultra diffuse galaxy. Ultra-diffuse galaxies have higher proportions ofglobular clusters than other galaxies, but NGC 5846 is one of the most extreme, with about 13% of its luminosity coming from globular clusters.[24]
NGC 5846 is the foremost galaxy of the largegalaxy group known as the NGC 5846 group. Other members of the group includeNGC 5813,NGC 5831,NGC 5845, andNGC 5854.[25] The group has two subgroups, one centered around the elliptical NGC 5813 and the other around NGC 5846, lying at a projected separation of 600 kpc.[22] The group is part of the Virgo III Groups, a very obvious chain of galaxy groups on the left side of the Virgo cluster, stretching across 40 million light years of space.[26]
This article contains quotations from this source, which is available under theCreative Commons Attribution 3.0 Unported (CC BY 3.0) license.
